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arXiv · 2609.00200

Gravitational waves from core collapse of rotating very-massive stars: 3D numerical relativity computation

Alan Tsz-Lok Lam·Masaru Shibata·Sho Fujibayashi
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Abstract

We numerically study the collapse of rotating, very-massive stellar cores with masses of $\approx 200$, $300$, $500$, and $1100M_\odot$ into black holes using both axisymmetric and three-dimensional (3D) numerical relativity. Our results indicate that when the dimensionless spin of the resulting black hole exceeds 0.8, a massive disk consistently forms around it. These massive, compact disks, carrying more than about 10\% of the black hole's mass, are prone to non-axisymmetric deformations that trigger gravitational-wave bursts with frequencies around 10-50 Hz. Such waves could be detected by the Einstein Telescope and Cosmic Explorer, even from sources a few Gpc away. We also summarize the gravitational-wave signals from axisymmetric collapse, which tend to have lower amplitudes and higher frequencies than those caused by non-axisymmetric instabilities.

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Alan Tsz-Lok Lam, Masaru Shibata, Sho Fujibayashi. 2026-08-31. Gravitational waves from core collapse of rotating very-massive stars: 3D numerical relativity computation. https://arxiv.org/abs/2609.00200

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